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Strongly interacting massive particle

A strongly interacting massive particle (SIMP) is a hypothetical particle that interacts strongly between themselves and weakly with ordinary matter, but could form the inferred dark matter despite this.[1][2][3]

Strongly interacting massive particles have been proposed as a solution for the ultra-high-energy cosmic-ray problem[4][5] and the absence of cooling flows in galactic clusters.[6][7]

Various experiments and observations have set constraints on SIMP dark matter from 1990 onward.[8][9][10][11][12][13]

SIMP annihilations would produce significant heat. DAMA set limits with NaI(Tl) crystals.[11][citation needed]

Measurements of Uranus's heat excess exclude SIMPs from 150 MeV to 104 GeV.[14] Earth's heat flow significantly constrains any cross section.[15]

  1. ^ Wandelt, Benjamin D; Dave, Romeel; Farrar, Glennys R; McGuire, Patrick C; Spergel, David N; Steinhardt, Paul J (2000), "Self-Interacting Dark Matter", in Cline, David B (ed.), Sources and Detection of Dark Matter and Dark Energy in the Universe, Springer-Verlag, p. 263, arXiv:astro-ph/0006344, Bibcode:2001sddm.symp..263W, ISBN 978-3-540-41216-8
  2. ^ Massey, Richard; et al. (2017), "Dark matter dynamics in Abell 3827: new data consistent with standard Cold Dark Matter", Monthly Notices of the Royal Astronomical Society, 477 (1): 669–677, arXiv:1708.04245, Bibcode:2018MNRAS.477..669M, doi:10.1093/mnras/sty630
  3. ^ Grossman, Lisa (April 5, 2018). "Dark matter isn't interacting with itself after all". ScienceNews. Retrieved 2018-04-05.
  4. ^ Chung, Daniel J. H; Farrar, Glennys R; Kolb, Edward W (1998), "Are ultrahigh energy cosmic rays signals of supersymmetry?", Physical Review D, 57 (8): 4606, arXiv:astro-ph/9707036, Bibcode:1998PhRvD..57.4606C, doi:10.1103/PhysRevD.57.4606, S2CID 44780458
  5. ^ Albuquerque, Ivone F. M; Farrar, Glennys R; Kolb, Edward W (1998), "Exotic massive hadrons and ultra-high energy cosmic rays", Physical Review D, 59 (1): 015021, arXiv:hep-ph/9805288, Bibcode:1998PhRvD..59a5021A, doi:10.1103/PhysRevD.59.015021
  6. ^ Qin, Bo; Wu, Xiang-Ping (2001), "Constraints on the Interaction between Dark Matter and Baryons from Cooling Flow Clusters", Physical Review Letters, 87 (6): 061301, arXiv:astro-ph/0106458, Bibcode:2001PhRvL..87f1301Q, doi:10.1103/PhysRevLett.87.061301, PMID 11497819, S2CID 13510283
  7. ^ Chuzhoy, Leonid; Nusser, Adi (2006), "Consequences of short range interactions between dark matter and protons in galaxy clusters", The Astrophysical Journal, 645 (2): 950–954, arXiv:astro-ph/0408184, Bibcode:2006ApJ...645..950C, doi:10.1086/504505, S2CID 16131656
  8. ^ Starkman, Glenn D; Gould, Andrew; Esmailzadeh, Rahim; Dimopoulos, Savas (1990), "Opening the window on strongly interacting dark matter", Physical Review D, 41 (12): 3594–3603, Bibcode:1990PhRvD..41.3594S, doi:10.1103/PhysRevD.41.3594, PMID 10012303
  9. ^ Cyburt, Richard H; Fields, Brian D; Pavlidou, Vasiliki; Wandelt, Benjamin D (2002), "Constraining Strong Baryon-Dark Matter Interactions with Primordial Nucleosynthesis and Cosmic Rays", Physical Review D, 65 (12): 123503, arXiv:astro-ph/0203240, Bibcode:2002PhRvD..65l3503C, doi:10.1103/PhysRevD.65.123503, S2CID 14926247.
  10. ^ Zaharijas, Gabrijela; Farrar, Glennys R (2004), "A Window in the Dark Matter Exclusion Limits", Physical Review D, 72 (8): 083502, arXiv:astro-ph/0406531, Bibcode:2005PhRvD..72h3502Z, doi:10.1103/PhysRevD.72.083502, S2CID 39245145
  11. ^ a b Bacci, C.; et al. (1996), "Improved limits on strongly interacting massive particles with NaI(Tl) scintillators", Astroparticle Physics, 4 (3): 195–198, Bibcode:1996APh.....4..195B, doi:10.1016/0927-6505(95)00032-1
  12. ^ McGuire, Patrick C; Steinhardt, Paul J (2001), "Cracking Open the Window for Strongly Interacting Massive Particles as the Halo Dark Matter", Proceedings of the International Cosmic Ray Conference, vol. 4, Hamburg, Germany, p. 1566, arXiv:astro-ph/0105567, Bibcode:2001ICRC....4.1566M{{cite book}}: CS1 maint: location missing publisher (link)
  13. ^ Javorsek II, D; Fischbach, E; Teplitz, V (2002), "New Experimental Bounds on the Contributions to the Cosmological Density Parameter Ω from Strongly Interacting Massive Particles", The Astrophysical Journal, 568 (1): 1–8, Bibcode:2002ApJ...568....1J, doi:10.1086/338796
  14. ^ Mitra, Saibal (2004), "Uranus's anomalously low excess heat constrains strongly interacting dark matter", Physical Review D, 70 (10): 103517, arXiv:astro-ph/0408341, Bibcode:2004PhRvD..70j3517M, doi:10.1103/PhysRevD.70.103517, S2CID 53396770
  15. ^ Mack, Gregory D; Beacom, John F; Bertone, Gianfranco (2007), "Towards Closing the Window on Strongly Interacting Dark Matter: Far-Reaching Constraints from Earth's Heat Flow", Physical Review D, 76 (4): 043523, arXiv:0705.4298, Bibcode:2007PhRvD..76d3523M, doi:10.1103/PhysRevD.76.043523, S2CID 119710504

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